We then generated an HMXB in the vicinity of that cluster at a random position picked from a Gaussian of width corresponding to the radius of the cluster, clipped at 3\(\sigma \) . We also imprinted to it a peculiar velocity drawn the same way as we do for the cluster, although the average of the Gaussian drawing was set at the cluster's velocity instead of the Galactic co-rotation speed. The width, still set at 15 km.s\(^{-1}\) ,is probably overestimated as [1]} also argue that it might be broadened by the orbital motion of binaries present in the clusters.
